While \(XRISM\)  and \(Athena\)  will lead to significant advancements in our understanding of the precise chemical make-up of the centers of galaxy groups and its redshift evolution, the high spectral resolution IFUs onboard both of these future missions have a limited field of view. This means that studies of the metal abundance ratios in the outskirts of groups and clusters would be very expensive in terms of observing time: nearby objects would be too large on the sky, and require mosaics composed of an unwieldy number of pointings, while high-redshift objects whose outskirts do fit within the FoV would be significantly dimmer. To give a concrete example, covering the entire area between 1–1.5 \(R_{500}\)  of NGC 5846for the \(R_{500}\)  value in [1]} would require no less than 423 observations with the \(Athena\) /X-IFU.
